Cosmology and particle physics
|
|
- Emery Garrison
- 5 years ago
- Views:
Transcription
1 Cosmology and particle physics Lecture notes Timm Wrase Lecture 5 The thermal universe - part I In the last lecture we have shown that our very early universe was in a very hot and dense state. During the expansion of the universe this hot soup cooled and underwent a variety of interesting transitions. In the next few lectures we will discuss the thermodynamical evolution of our universe from a split second after the big bang until the release of the cosmic microwave background 380,000 years after the big bang. We will from now on set the Boltzmann constant equal to one k B = 1 and measure temperatures in ev. 1 The Standard Model of Particle Physics Currently the world s largest particle accelerator, the Large Hadron Collider, does experiments at an energy of up to 13 T ev. So we understand particle physics up to this energy scale very well. The particles with masses below this scale and their interactions are described by the so called standard model of particle physics, which is a particular quantum field theory. Here we will recall some features of the standard model of particle physics and summarize the relevant terminology before we discuss particle physics in the early universe. Compared to the periodic table that you are probably familiar with from your chemistry class, the content of the standard model of particle physics is fairly simple. We know in total of 13 different particles that constitute all the matter in the standard model of particle physics. These 13 particles interact via three different forces: The electro-magnetic force, the weak force and the strong force, which we will all discuss below. 1.1 The (known) particles in our universe The 13 particles come in three different groups: 1. The six leptons are probably the particles you are most familiar with. They are fermions and have spin 1. They consist of the electron and its cousins the µ- and τ-particle that 2 all carry one unit of negative electric charge. Additionally there are three neutrinos that are called ν e, ν µ and ν τ and that all are electrically neutral. All these six leptons are uncharged under the strong force but they do interact via the weak force. 2. There are six more fermionic spin 1 particles that are called quarks. These quarks 2 combine to form the probably more familiar protons and neutrons as well as other particles that we will discuss below. The quarks also come in two groups of three particles: the up, charm and top quarks carry + 2 units of electrical charge and the 3 1
2 down, strange and bottom quarks carry 1 unit of electric charge. All quarks are 3 charged under the strong force and the weak force. 3. Lastly there is one more particle in the standard model that was predicted a long time ago but only recently discovered in 2012, the Higgs boson which has spin-0. The Higgs particle plays a special role among all particles. It is responsible for giving a mass to the other particles. This process of giving a mass involves a phase transition in our very early universe. This phase transition changes the cosmological constant we discussed last time by a term that is of the order λ Higgs This means that the value of the cosmological constant before this transition λ before needs to cancel with λ Higgs precisely to 55 digits so that λ today λ before + λ Higgs. All these particles and their masses are shown in figure 1. Figure 1: The known particles in our universe (taken from Wikipedia). Interestingly the leptons and quarks come both in three families (the first three columns in figure 1). Each family contains four particles with the same charges but with different masses. Since the heavier particles in the second and third family can decay into the lighter particles in the first family, it turns out that essentially all standard model particles in our 1 universe are the particles from the first column. This means in particular that all the elements in the periodic table are made up of only of three different particles: the electron, and the up and down quarks. 1 Neutrinos can oscillate between different families and heavier particles can be created in processes that involve energies larger than their rest mass but these heavier particles quickly decay to up and down quarks and/or electrons. 2
3 1.2 The three forces in the standard model of particle physics There are four particles that control the interactions between these 13 particles. The three different interactions in the standard model of particle physics are mediated by bosonic spin 1 particles and we quickly discuss the three interactions: The electro-magnetic force The force you are probably most familiar with is the electro-magnetic force that is mediated by photons. Many of the particles in the standard model carry an electric charge and therefore interact with photons. Since the photon is massless the interaction strength between two particles falls off as a power law (versus an exponential). This means that the electro-magnetic force could compete with gravity which has the same power law fall off and is in some sense much weaker. However, our universe is essentially electrically neutral on all but very small scales. So for example the earth and the sun carry essentially no net electric charge so their interaction is only determined by their masses, i.e. by gravity, and the electro-magnetic force plays no role. The same is true on larger scales that are relevant for cosmology. The weak force The weak interaction is probably the force you are most unfamiliar with. It is mediated by three different particles: the electrically neutral Z boson and the two electrically charged W ± bosons, where the later carry ±1 unit of electric charge. Since these three particles that mediate the weak force are rather heavy, the weak force is relevant only on fairly short distances, smaller than m, like inside a nucleus. There the weak force is responsible for radioactive decay of nuclei. The strong force The strong force is what keeps for example the positively charged protons together inside the nuclei. So it is clear that it is much stronger than the electric force between these charged particles. At low energies the strong force becomes so strong that charged particles cannot exist in isolation. Whenever we try to separate two particles that are charged under the strong force, the energy in the field between the particles becomes so large that it can lead to pair production of new particles that combine with the particles we tried to separate into particles that are neutral under the strong force. The strong force is different from the electromagnetic force in the sense that there are three different types of charges (plus their anti-charges carried by the anti-particles). So we cannot label the charges by a positive or negative number but rather we have to use three different labels (and anti-labels). For lack of a better label people call the three charges red, green and blue (and the corresponding anti-charges anti-red, anti-green and anti-blue). All quarks carry a single color charge, i.e. they come in three types so that for example we have a red, a green and a blue up quark. To form particles that are neutral under the strong force we need all three colors to appear once or we can combine a color with an anti-color. 3
4 1.3 Hadrons, baryons and mesons Since the quarks are not playing much of a role in our everyday life, let us discuss a little bit more how they form more familiar composite particles, which also allows us to introduce a little bit more terminology. Above we discussed the six leptons, the electron, muon and tau and the three corresponding neutrinos. The name lepton is derived from a Greek word that means fine, thin, little, which is appropriate since, as far as we know, these particles are fundamental in the sense that they are not composed of other particles. The leptons are supposed to be contrasted with the hadrons, derived from the Greek word for thick and strong. These are not fundamental particles but rather particles that are kept together by the strong force. These hadrons are furthermore divided into mesons, which are bosonic particles with integer spin and baryons, which are fermionic particles with half integer spin. Let us try to build some baryons. As we have heard above, the quarks have to appear in color neutral bound states at low energies. So we cannot get a baryon that is made up of a single quarks. In order to half integer spin, i.e. a baryon, we therefore need three quarks (and no anti-quarks). If we take three quarks of the same type, like for example three up quarks, then they cannot combine due to the fermi statistics. Since the quarks are spin 1 2 particles we can combine at most one spin + 1 quark and one spin 1 quark of the same 2 2 type. So the lightest baryon is a composite particle of two up quarks and one down quark, often denoted as uud. This baryon has electric charge +1 and is called the proton. One might think that each of the three quarks can have different color charges so there should be more than one proton, however, this is not the case since color neutrality requires us to take the antisymmetric combination of all color neutral combinations of the three quarks. The proton is as far as we know the only stable baryon. The next heavier baryon is udd. It is the electrically neutral neutron, that has a mean lifetime of slightly less than 15 minutes. These two baryons will play a very important role in the creation of nuclei in our very early universe, as we will discuss in lecture 8. All other baryons have a very short lifetime so that they quickly decay into protons and neutrons. The mesons are all unstable so they do not play such an important role in cosmology. Let us nevertheless discuss the pions that are the lightest mesons: We want to get a particle with integer spin so we need (at least) two quarks to construct a meson. Since we want these particles to be color neutral we need actually a quark and an anti-quark to construct the simplest and lightest mesons. Restricting again to hadrons formed out of the u and d quarks and anti-quarks we seem to have four possibilities to construct two quark mesons: uū, d d, u d and ūd, where a bar over a quark denotes the anti-quark. However, the actual meson particles we observe are sometimes linear combinations of quark-anti-quark pairs. In particular the sum of uū and d d combines with ±s s to form two η mesons. This leaves us with only three light π mesons that are made up of u and d quarks and anti-quarks: The π 0 = (uū d d)/ 2, the π + = u d and the π = ūd, where the superscript denotes the electric charges in units of the electron charge. All these mesons decay very quickly with a mean lifetime of s for the π ± and s for the π 0. 4
5 1.4 Gravity and a theory of everything Note, that the standard model or particle physics neglects gravity entirely. This is very well justified in most regimes of interest to elementary particle physics but it tells us that in order to describe our entire universe, we need another theory that unifies quantum field theories with gravity in a so called theory of everything. General relativity that we are using in this course to describe the evolution of our universe is likewise incomplete since it is a classical theory and it inevitably breaks down near the Planck scale M P which is given by M P = 1 8πG = GeV. (1) Since the universe was at higher and higher temperatures/energies the further back in time we are going, we reach a point at which general relativity cannot be used anymore. This in particular means we cannot use general relativity to understand the actual beginning of our universe, i.e. the big bang. It is also unclear whether we will ever be able to get experimental insight into the physics that caused the big bang. However, between the energies of less than an ev at the time the CMB was released until the energies studied in particle accelerators of a few T ev we have 12 orders of magnitude of well understood physics to discuss and from the T ev range up to the Planck scale we will discuss another 15 orders of magnitude in energy of slightly more speculative physics. There are also ideas for theories of quantum gravity that go beyond general relativity and might allow us to theoretically understand the initial singularity that arises in general relativity at the beginning of our universe. 2 The universe in thermal equilibrium In the early universe at temperatures above a few hundred GeV all standard model particles will have energies that are much larger than their rest mass: E(p) = m 2 + p 2 p. (2) This means that they do not behave like non-relativistic (pressureless) matter but rather like radiation (i.e. like for example photons for which E = p). Since the masses are negligible in this era, there is only one scale in the standard model which is the rate of interactions Γ, i.e. the number of interactions per time. In principle this rate can be different for the different particles but we neglect this for the rough estimates in this section. In our expanding universe there is one more length or time scale set by the Hubble scale H. If the particles interact a lot without feeling the expansion of the universe, then they will be in local equilibrium. This would mean that Γ H. (3) If the above equation is true, then we can use equilibrium thermodynamics to describe our universe. We would therefore like to estimate during which temperatures/energies the above is expected to be true. The particle interaction rate can be written as Γ nσv, (4) 5
6 where n is the number density, i.e. the number of particles per volume, σ is the interaction cross-section and v is the average velocity of the particles. Since, as we argued above, all particles are highly relativistic for T 100GeV, we have v c = 1. The only dimensionful quantity is the temperature T, that has the dimension of an energy which is the same as an inverse length. So we find for the number density and the cross section n T 3, σ T 2. (5) For the cross section we can be more precise. Two particles interact dominantly via the exchange of one of the gauge bosons (that are all massless above 100GeV ). We often write this in terms of Feynman diagrams that use straight lines to indicate fermions and wiggly lines to describe a gauge boson: The interaction cross section is the square of such a diagram so that it goes like the fourth power of the interaction strength between the fermion and the gauge boson. This interaction strength is usually called α, which gives σ α2 T 2. (6) Putting this together we find the following scaling of the interaction rate Γ nσ α 2 T. (7) The actual value of α depends on the particular force with which the particles interact as well as the energy scale. However, at high energies the interaction strengths of all forces seem to become almost the same, which hints at a unification of all force in a so called grand unified theory (GUT). At this GUT scale the energy is approximately GeV and the value of α is α.05. As we have seen last time, our early universe was dominated by radiation. 2 This means that H 2 = ρ 1 T 4 H T 2. (8) 3MP 2 a(t) 4 MP 2 MP 2 M P Putting this together we find that Γ H α2 M P T 1016 GeV T, (9) which means for roughly 100GeV T GeV we have Γ H. So our early and hot universe was in a state of local equilibrium and we can describe it using equilibrium thermodynamics. 2 This is also plausible from the above discussion that showed that all the standard model particles behaved like radiation instead of matter in the early universe. 6
7 Baryogenesis In the following we will describe the cooling of our universe starting from a soup of matter and photons at a temperature of a few hundred GeV, using our knowledge of particle physics and thermodynamics. However, before we do that let us mention a puzzle: In a very hot universe we can create particle-anti-particle pairs from photons, denoted γ. For example for the electron e and the positron e + we can have the reversible process e + e + γ + γ. (10) In an expanding universe we know that the photons lose energy due to the redshift. This means that there is a certain point at which the two photons on the right won t have enough energy to create an electron-positron pair. At that moment the above process should only go in one direction e + e + γ + γ. (11) If the early universe has an equal number of particles and anti-particles then eventually we would expect that all particles and anti-particles annihilate and leave a universe filled with photons. However, in our universe there is an asymmetry between matter and anti-matter, so that our universe ended up with matter and not just radiation. This asymmetry can be quantified by the ratio between the number of baryons (protons and neutrons) and photons in our current universe. Observation tell us that today n b n γ 10 9, (12) while the same ratio for anti-baryons seems to be essentially zero. There is no mechanism inside the standard model of particle physics that can explain this so called baryogenesis, i.e. the observed matter-anti-matter asymmetry, so we will simply assume that the initial conditions of the universe were such that they lead to the observed baryon to photon ratio. 3 3 There are a variety of theoretical ideas of how such an asymmetry can arise but so far the experiments have not singled out any particular model, so we refrain from discussing baryogenesis in any further detail. 7
Earlier in time, all the matter must have been squeezed more tightly together and a lot hotter AT R=0 have the Big Bang
Re-cap from last lecture Discovery of the CMB- logic From Hubble s observations, we know the Universe is expanding This can be understood theoretically in terms of solutions of GR equations Earlier in
More informationChapter 32 Lecture Notes
Chapter 32 Lecture Notes Physics 2424 - Strauss Formulas: mc 2 hc/2πd 1. INTRODUCTION What are the most fundamental particles and what are the most fundamental forces that make up the universe? For a brick
More informationLecture 2: The First Second origin of neutrons and protons
Lecture 2: The First Second origin of neutrons and protons Hot Big Bang Expanding and cooling Soup of free particles + anti-particles Symmetry breaking Soup of free quarks Quarks confined into neutrons
More informationAn Introduction to Particle Physics
An Introduction to Particle Physics The Universe started with a Big Bang The Universe started with a Big Bang What is our Universe made of? Particle physics aims to understand Elementary (fundamental)
More informationNuclear and Particle Physics 3: Particle Physics. Lecture 1: Introduction to Particle Physics February 5th 2007
Nuclear and Particle Physics 3: Particle Physics Lecture 1: Introduction to Particle Physics February 5th 2007 Particle Physics (PP) a.k.a. High-Energy Physics (HEP) 1 Dr Victoria Martin JCMB room 4405
More informationOverview. The quest of Particle Physics research is to understand the fundamental particles of nature and their interactions.
Overview The quest of Particle Physics research is to understand the fundamental particles of nature and their interactions. Our understanding is about to take a giant leap.. the Large Hadron Collider
More information9.2.E - Particle Physics. Year 12 Physics 9.8 Quanta to Quarks
+ 9.2.E - Particle Physics Year 12 Physics 9.8 Quanta to Quarks + Atomic Size n While an atom is tiny, the nucleus is ten thousand times smaller than the atom and the quarks and electrons are at least
More informationLecture 02. The Standard Model of Particle Physics. Part I The Particles
Lecture 02 The Standard Model of Particle Physics Part I The Particles The Standard Model Describes 3 of the 4 known fundamental forces Separates particles into categories Bosons (force carriers) Photon,
More informationTHERMAL HISTORY OF THE UNIVERSE
M. Pettini: Introduction to Cosmology Lecture 7 THERMAL HISTORY OF THE UNIVERSE The Universe today is bathed in an all-pervasive radiation field, the Cosmic Microwave Background (CMB) which we introduced
More information1. What does this poster contain?
This poster presents the elementary constituents of matter (the particles) and their interactions, the latter having other particles as intermediaries. These elementary particles are point-like and have
More informationThe first one second of the early universe and physics beyond the Standard Model
The first one second of the early universe and physics beyond the Standard Model Koichi Hamaguchi (University of Tokyo) @ Colloquium at Yonsei University, November 9th, 2016. Credit: X-ray: NASA/CXC/CfA/M.Markevitch
More informationHot Big Bang model: early Universe and history of matter
Hot Big Bang model: early Universe and history of matter nitial soup with elementary particles and radiation in thermal equilibrium. adiation dominated era (recall energy density grows faster than matter
More informationPhysics 4213/5213 Lecture 1
August 28, 2002 1 INTRODUCTION 1 Introduction Physics 4213/5213 Lecture 1 There are four known forces: gravity, electricity and magnetism (E&M), the weak force, and the strong force. Each is responsible
More informationParticle Physics Outline the concepts of particle production and annihilation and apply the conservation laws to these processes.
Particle Physics 12.3.1 Outline the concept of antiparticles and give examples 12.3.2 Outline the concepts of particle production and annihilation and apply the conservation laws to these processes. Every
More informationMost of Modern Physics today is concerned with the extremes of matter:
Most of Modern Physics today is concerned with the extremes of matter: Very low temperatures, very large numbers of particles, complex systems Æ Condensed Matter Physics Very high temperatures, very large
More informationThe Standard Model. 1 st 2 nd 3 rd Describes 3 of the 4 known fundamental forces. Separates particle into categories
The Standard Model 1 st 2 nd 3 rd Describes 3 of the 4 known fundamental forces. Separates particle into categories Bosons (force carriers) Photon, W, Z, gluon, Higgs Fermions (matter particles) 3 generations
More informationTEACHER. The Atom 4. Make a drawing of an atom including: Nucleus, proton, neutron, electron, shell
Click on the SUBATOMIC roadmap button on the left. Explore the Subatomic Universe Roadmap to answer the following questions. Matter 1. What 3 atoms is a water molecule made of? Two Hydrogen atoms and one
More informationPhys 102 Lecture 28 Life, the universe, and everything
Phys 102 Lecture 28 Life, the universe, and everything 1 Today we will... Learn about the building blocks of matter & fundamental forces Quarks and leptons Exchange particle ( gauge bosons ) Learn about
More information1 Introduction. 1.1 The Standard Model of particle physics The fundamental particles
1 Introduction The purpose of this chapter is to provide a brief introduction to the Standard Model of particle physics. In particular, it gives an overview of the fundamental particles and the relationship
More informationMost of Modern Physics today is concerned with the extremes of matter:
Most of Modern Physics today is concerned with the extremes of matter: Very low temperatures, very large numbers of particles, complex systems Æ Condensed Matter Physics Very high temperatures, very large
More informationMatter: it s what you have learned that makes up the world Protons, Neutrons and Electrons
Name The Standard Model of Particle Physics Matter: it s what you have learned that makes up the world Protons, Neutrons and Electrons Just like there is good and evil, matter must have something like
More informationPHY-105: Introduction to Particle and Nuclear Physics
M. Kruse, Spring 2011, Phy-105 PHY-105: Introduction to Particle and Nuclear Physics Up to 1900 indivisable atoms Early 20th century electrons, protons, neutrons Around 1945, other particles discovered.
More informationThe Standard Model (part I)
The Standard Model (part I) Speaker Jens Kunstmann Student of Physics in 5 th year at Greifswald University, Germany Location Sommerakademie der Studienstiftung, Kreisau 2002 Topics Introduction The fundamental
More informationFundamental Particles
Fundamental Particles Standard Model of Particle Physics There are three different kinds of particles. Leptons - there are charged leptons (e -, μ -, τ - ) and uncharged leptons (νe, νμ, ντ) and their
More informationINTRODUCTION TO THE STANDARD MODEL OF PARTICLE PHYSICS
INTRODUCTION TO THE STANDARD MODEL OF PARTICLE PHYSICS Class Mechanics My office (for now): Dantziger B Room 121 My Phone: x85200 Office hours: Call ahead, or better yet, email... Even better than office
More informationReview Chap. 18: Particle Physics
Final Exam: Sat. Dec. 18, 2:45-4:45 pm, 1300 Sterling Exam is cumulative, covering all material Review Chap. 18: Particle Physics Particles and fields: a new picture Quarks and leptons: the particle zoo
More informationParticle Physics Lectures Outline
Subatomic Physics: Particle Physics Lectures Physics of the Large Hadron Collider (plus something about neutrino physics) 1 Particle Physics Lectures Outline 1 - Introduction The Standard Model of particle
More informationOption 212: UNIT 2 Elementary Particles
Department of Physics and Astronomy Option 212: UNIT 2 Elementary Particles SCHEDULE 26-Jan-15 13.00pm LRB Intro lecture 28-Jan-15 12.00pm LRB Problem solving (2-Feb-15 10.00am E Problem Workshop) 4-Feb-15
More informationModern Physics: Standard Model of Particle Physics (Invited Lecture)
261352 Modern Physics: Standard Model of Particle Physics (Invited Lecture) Pichet Vanichchapongjaroen The Institute for Fundamental Study, Naresuan University 1 Informations Lecturer Pichet Vanichchapongjaroen
More information1. Introduction. Particle and Nuclear Physics. Dr. Tina Potter. Dr. Tina Potter 1. Introduction 1
1. Introduction Particle and Nuclear Physics Dr. Tina Potter Dr. Tina Potter 1. Introduction 1 In this section... Course content Practical information Matter Forces Dr. Tina Potter 1. Introduction 2 Course
More informationCosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation
Cosmology Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Energy density versus scale factor z=1/a-1 Early times,
More informationLecture 36: The First Three Minutes Readings: Sections 29-1, 29-2, and 29-4 (29-3)
Lecture 36: The First Three Minutes Readings: Sections 29-1, 29-2, and 29-4 (29-3) Key Ideas Physics of the Early Universe Informed by experimental & theoretical physics Later stages confirmed by observations
More informationEssential Physics II. Lecture 14:
Essential Physics II E II Lecture 14: 18-01-16 Last lecture of EP2! Congratulations! This was a hard course. Be proud! Next week s exam Next Monday! All lecture slides on course website: http://astro3.sci.hokudai.ac.jp/~tasker/teaching/ep2
More informationPhysicsAndMathsTutor.com 1
Q1. (a) The K meson has strangeness 1. State the quark composition of a meson... State the baryon number of the K meson... (iii) What is the quark composition of the K meson?.... The figure below shows
More informationThe Big Bang Theory, General Timeline. The Planck Era. (Big Bang To 10^-35 Seconds) Inflationary Model Added. (10^-35 to 10^-33 Of A Second)
The Big Bang Theory, General Timeline The Planck Era. (Big Bang To 10^-35 Seconds) The time from the exact moment of the Big Bang until 10^-35 of a second later is referred to as the Planck Era. While
More informationMatter vs. Antimatter in the Big Bang. E = mc 2
Matter vs. Antimatter in the Big Bang Threshold temperatures If a particle encounters its corresponding antiparticle, the two will annihilate: particle + antiparticle ---> radiation * Correspondingly,
More informationLecture PowerPoint. Chapter 32 Physics: Principles with Applications, 6 th edition Giancoli
Lecture PowerPoint Chapter 32 Physics: Principles with Applications, 6 th edition Giancoli 2005 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
More informationTHE STANDARD MODEL OF MATTER
VISUAL PHYSICS ONLINE THE STANDARD MODEL OF MATTER The "Standard Model" of subatomic and sub nuclear physics is an intricate, complex and often subtle thing and a complete study of it is beyond the scope
More informationFUNDAMENTAL PARTICLES CLASSIFICATION! BOSONS! QUARKS! FERMIONS! Gauge Bosons! Fermions! Strange and Charm! Top and Bottom! Up and Down!
FUNDAMENTAL PARTICLES CLASSIFICATION! BOSONS! --Bosons are generally associated with radiation and are sometimes! characterized as force carrier particles.! Quarks! Fermions! Leptons! (protons, neutrons)!
More informationFundamental Particles and Forces
Fundamental Particles and Forces A Look at the Standard Model and Interesting Theories André Gras PHYS 3305 SMU 1 Overview Introduction to Fundamental Particles and Forces Brief History of Discovery The
More informationOption 212: UNIT 2 Elementary Particles
Department of Physics and Astronomy Option 212: UNIT 2 Elementary Particles SCHEDULE 26-Jan-15 13.pm LRB Intro lecture 28-Jan-15 12.pm LRB Problem solving (2-Feb-15 1.am E Problem Workshop) 4-Feb-15 12.pm
More informationParticle Physics. All science is either physics or stamp collecting and this from a 1908 Nobel laureate in Chemistry
Particle Physics JJ Thompson discovered electrons in 1897 Rutherford discovered the atomic nucleus in 1911 and the proton in 1919 (idea of gold foil expt) All science is either physics or stamp collecting
More informationPHYS 420: Astrophysics & Cosmology
PHYS 420: Astrophysics & Cosmology Dr Richard H. Cyburt Assistant Professor of Physics My office: 402c in the Science Building My phone: (304) 384-6006 My email: rcyburt@concord.edu My webpage: www.concord.edu/rcyburt
More informationQuantum Numbers. Elementary Particles Properties. F. Di Lodovico c 1 EPP, SPA6306. Queen Mary University of London. Quantum Numbers. F.
Elementary Properties 1 1 School of Physics and Astrophysics Queen Mary University of London EPP, SPA6306 Outline Most stable sub-atomic particles are the proton, neutron (nucleons) and electron. Study
More informationElementary Particle Physics Glossary. Course organiser: Dr Marcella Bona February 9, 2016
Elementary Particle Physics Glossary Course organiser: Dr Marcella Bona February 9, 2016 1 Contents 1 Terms A-C 5 1.1 Accelerator.............................. 5 1.2 Annihilation..............................
More informationSome fundamental questions
Some fundamental questions What is the standard model of elementary particles and their interactions? What is the origin of mass and electroweak symmetry breaking? What is the role of anti-matter in Nature?
More informationChapter 27 The Early Universe Pearson Education, Inc.
Chapter 27 The Early Universe Units of Chapter 27 27.1 Back to the Big Bang 27.2 The Evolution of the Universe More on Fundamental Forces 27.3 The Formation of Nuclei and Atoms 27.4 The Inflationary Universe
More informationWesley Smith, U. Wisconsin, January 21, Physics 301: Introduction - 1
Wesley Smith, U. Wisconsin, January 21, 2014 Physics 301: Introduction - 1 Physics 301: Physics Today Prof. Wesley Smith, wsmith@hep.wisc.edu Undergraduate Physics Colloquium! Discussions of current research
More informationA few thoughts on 100 years of modern physics. Quanta, Quarks, Qubits
A few thoughts on 100 years of modern physics Quanta, Quarks, Qubits Quanta Blackbody radiation and the ultraviolet catastrophe classical physics does not agree with the observed world Planck s idea: atoms
More informationKatsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy
11/14/12 Katsushi Arisaka 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Seven Phases of Cosmic Evolution 11/14/12 Katsushi Arisaka
More informationASTR 101 General Astronomy: Stars & Galaxies
ASTR 101 General Astronomy: Stars & Galaxies ANNOUNCEMENTS FINAL EXAM: THURSDAY, May 14 th, 11:15am Last Astronomy public talk, May 8 th (up to 3% Extra class credit (see Blackboard announcement for details)
More informationChapter 22: Cosmology - Back to the Beginning of Time
Chapter 22: Cosmology - Back to the Beginning of Time Expansion of Universe implies dense, hot start: Big Bang Future of universe depends on the total amount of dark and normal matter Amount of matter
More informationCosmology and particle physics
Cosmology and particle physics Lecture notes Timm Wrase Lecture 9 Inflation - part I Having discussed the thermal history of our universe and in particular its evolution at times larger than 10 14 seconds
More informationClass 18 The early universe and nucleosynthesis
Class 18 The early universe and nucleosynthesis ch 12 of book Why did Gamov and Peebles suggest hot big band model? If the early Universe was hot (full of energy), a lot of features of the current universe
More informationA first trip to the world of particle physics
A first trip to the world of particle physics Itinerary Massimo Passera Padova - 13/03/2013 1 Massimo Passera Padova - 13/03/2013 2 The 4 fundamental interactions! Electromagnetic! Weak! Strong! Gravitational
More informationThe Scale-Symmetric Theory as the Origin of the Standard Model
Copyright 2017 by Sylwester Kornowski All rights reserved The Scale-Symmetric Theory as the Origin of the Standard Model Sylwester Kornowski Abstract: Here we showed that the Scale-Symmetric Theory (SST)
More informationFundamental Forces. David Morrissey. Key Concepts, March 15, 2013
Fundamental Forces David Morrissey Key Concepts, March 15, 2013 Not a fundamental force... Also not a fundamental force... What Do We Mean By Fundamental? Example: Electromagnetism (EM) electric forces
More information.! " # e " + $ e. have the same spin as electron neutrinos, and is ½ integer (fermions).
Conservation Laws For every conservation of some quantity, this is equivalent to an invariance under some transformation. Invariance under space displacement leads to (and from) conservation of linear
More informationSaturday Morning Physics -- Texas A&M University. What is Matter and what holds it together? Dr. Rainer J. Fries. January 27, 2007
Saturday Morning Physics -- Texas A&M University Particles and Forces What is Matter and what holds it together? Dr. Rainer J. Fries January 27, 2007 Zooming in on the World around us Particles and Forces
More informationSaturday Morning Physics -- Texas A&M University Dr. Rainer J. Fries
Saturday Morning Physics -- Texas A&M University Particles and Forces What is Matter and what holds it together? Dr. Rainer J. Fries January 27, 2007 Zooming in on the World around us Particles and Forces
More informationCosmology and particle physics
Fedora GNU/Linux; LATEX 2ɛ; xfig Cosmology and particle physics Mark Alford Washington University Saint Louis, USA Outline I Particle physics: What the universe is made of. quarks, leptons, and the forces
More informationOrigin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean?
Origin of the Universe - 2 ASTR 2120 Sarazin What does it all mean? Fundamental Questions in Cosmology 1. Why did the Big Bang occur? 2. Why is the Universe old? 3. Why is the Universe made of matter?
More informationParticle Physics (concise summary) QuarkNet summer workshop June 24-28, 2013
Particle Physics (concise summary) QuarkNet summer workshop June 24-28, 2013 1 Matter Particles Quarks: Leptons: Anti-matter Particles Anti-quarks: Anti-leptons: Hadrons Stable bound states of quarks Baryons:
More informationChapter 22 Lecture. The Cosmic Perspective. Seventh Edition. The Birth of the Universe Pearson Education, Inc.
Chapter 22 Lecture The Cosmic Perspective Seventh Edition The Birth of the Universe The Birth of the Universe 22.1 The Big Bang Theory Our goals for learning: What were conditions like in the early universe?
More informationFACULTY OF SCIENCE. High Energy Physics. WINTHROP PROFESSOR IAN MCARTHUR and ADJUNCT/PROFESSOR JACKIE DAVIDSON
FACULTY OF SCIENCE High Energy Physics WINTHROP PROFESSOR IAN MCARTHUR and ADJUNCT/PROFESSOR JACKIE DAVIDSON AIM: To explore nature on the smallest length scales we can achieve Current status (10-20 m)
More informationElectron-positron pairs can be produced from a photon of energy > twice the rest energy of the electron.
Particle Physics Positron - discovered in 1932, same mass as electron, same charge but opposite sign, same spin but magnetic moment is parallel to angular momentum. Electron-positron pairs can be produced
More informationPhysics 661. Particle Physics Phenomenology. October 9, Physics 661, lecture 5 1
Physics 661 Particle Physics Phenomenology October 9, 2001 Physics 661, lecture 5 1 Outline Quarks and Leptons Unfinished discussion: the interstellar magnetic field Elem. Part. and High Energy Physics
More informationParticles and Forces
Particles and Forces Particles Spin Before I get into the different types of particle there's a bit more back story you need. All particles can spin, like the earth on its axis, however it would be possible
More informationDEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS
DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS LSN 7-3: THE STRUCTURE OF MATTER Questions From Reading Activity? Essential Idea: It is believed that all the matter around us is made up of fundamental
More informationPhysicsAndMathsTutor.com
OR K π 0 + µ + v ( µ ) M. (a) (i) quark antiquark pair OR qq OR named quark antiquark pair 0 (iii) us (b) (i) Weak any of the following also score mark: weak interaction weak interaction force weak nuclear
More informationChapter 46. Particle Physics and Cosmology
Chapter 46 Particle Physics and Cosmology Atoms as Elementary Particles Atoms From the Greek for indivisible Were once thought to be the elementary particles Atom constituents Proton, neutron, and electron
More informationFinish up our overview of small and large
Finish up our overview of small and large Lecture 5 Limits of our knowledge Clicker practice quiz Some terminology... "Elementary particles" = objects that make up atoms (n,p,e) or are produced when atoms
More informationThe Four Fundamental Forces. The Four Fundamental Forces. Gravitational Force. The Electrical Force. The Photon (γ) Unification. Mass.
The Four Fundamental Forces What are the four fundamental forces? The Four Fundamental Forces What are the four fundamental forces? Weaker Stronger Gravitational, Electromagnetic, Strong and Weak Nuclear
More informationcgrahamphysics.com Particles that mediate force Book pg Exchange particles
Particles that mediate force Book pg 299-300 Exchange particles Review Baryon number B Total # of baryons must remain constant All baryons have the same number B = 1 (p, n, Λ, Σ, Ξ) All non baryons (leptons
More informationParticle + Physics at ATLAS and the Large Hadron Coillder
Particle + Physics at ATLAS and the Large Hadron Coillder Discovering the elementary particles of the Universe Kate Shaw The International Centre for Theoretical Physics + Overview Introduction to Particle
More informationParticle physics: what is the world made of?
Particle physics: what is the world made of? From our experience from chemistry has told us about: Name Mass (kg) Mass (atomic mass units) Decreasing mass Neutron Proton Electron Previous lecture on stellar
More information32 IONIZING RADIATION, NUCLEAR ENERGY, AND ELEMENTARY PARTICLES
32 IONIZING RADIATION, NUCLEAR ENERGY, AND ELEMENTARY PARTICLES 32.1 Biological Effects of Ionizing Radiation γ-rays (high-energy photons) can penetrate almost anything, but do comparatively little damage.
More informationChapter 22 Back to the Beginning of Time
Chapter 22 Back to the Beginning of Time Expansion of Universe implies dense, hot start: Big Bang Back to the Big Bang The early Universe was both dense and hot. Equivalent mass density of radiation (E=mc
More informationChapter 27: The Early Universe
Chapter 27: The Early Universe The plan: 1. A brief survey of the entire history of the big bang universe. 2. A more detailed discussion of each phase, or epoch, from the Planck era through particle production,
More informationASTR 1120 General Astronomy: Stars & Galaxies. OUR Universe: Accelerating Universe
ASTR 1120 General Astronomy: Stars & Galaxies FINAL: Saturday, Dec 12th, 7:30pm, HERE ALTERNATE FINAL: Monday, Dec 7th, 5:30pm in Muenzinger E131 Last OBSERVING session, Tue, Dec.8th, 7pm Please check
More informationPlasma Universe. The origin of CMB
Plasma Universe As we go back in time, temperature goes up. T=2.73(1+z) K At z~1100, T~3000 K About the same temperature as M-dwarfs Ionization of hydrogen atoms H + photon! p + e - Inverse process: recombination
More informationParticles in the Early Universe
Particles in the Early Universe David Morrissey Saturday Morning Physics, October 16, 2010 Using Little Stuff to Explain Big Stuff David Morrissey Saturday Morning Physics, October 16, 2010 Can we explain
More informationElementary particles, forces and Feynman diagrams
Elementary particles, forces and Feynman diagrams Particles & Forces quarks Charged leptons (e,µ,τ) Neutral leptons (ν) Strong Y N N Electro Magnetic Y Y N Weak Y Y Y Quarks carry strong, weak & EM charge!!!!!
More informationParticle Physics: Problem Sheet 5
2010 Subatomic: Particle Physics 1 Particle Physics: Problem Sheet 5 Weak, electroweak and LHC Physics 1. Draw a quark level Feynman diagram for the decay K + π + π 0. This is a weak decay. K + has strange
More informationGravitational Repulsion of Matter and Antimatter
Gravitational Repulsion of Matter and Antimatter The changing acceleration of the electrons explains the created negative electric field of the magnetic induction, the electromagnetic inertia, the changing
More informationThe first 400,000 years
The first 400,000 years All about the Big Bang Temperature Chronology of the Big Bang The Cosmic Microwave Background (CMB) The VERY early universe Our Evolving Universe 1 Temperature and the Big Bang
More informationGeneral and Inorganic Chemistry I.
General and Inorganic Chemistry I. Lecture 2 István Szalai Eötvös University István Szalai (Eötvös University) Lecture 2 1 / 44 Outline 1 Introduction 2 Standard Model 3 Nucleus 4 Electron István Szalai
More informationThe Dark Side of the Higgs Field and General Relativity
The Dark Side of the Higgs Field and General Relativity The gravitational force attracting the matter, causing concentration of the matter in a small space and leaving much space with low matter concentration:
More informationWe can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years
² ² ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter:
More informationNeutrino Physics. Kam-Biu Luk. Tsinghua University and University of California, Berkeley and Lawrence Berkeley National Laboratory
Neutrino Physics Kam-Biu Luk Tsinghua University and University of California, Berkeley and Lawrence Berkeley National Laboratory 4-15 June, 2007 Outline Brief overview of particle physics Properties of
More informationHigh Energy Physics. QuarkNet summer workshop June 24-28, 2013
High Energy Physics QuarkNet summer workshop June 24-28, 2013 1 The Birth of Particle Physics In 1896, Thompson showed that electrons were particles, not a fluid. In 1905, Einstein argued that photons
More informationAstronomy, Astrophysics, and Cosmology
Astronomy, Astrophysics, and Cosmology Luis A. Anchordoqui Department of Physics and Astronomy Lehman College, City University of New York Lesson IX April 12, 2016 arxiv:0706.1988 L. A. Anchordoqui (CUNY)
More informationThe Goals of Particle Physics
The Goals of Particle Physics Richard (Ryszard) Stroynowski Department of Physics Southern Methodist University History of Elementary Particles Science as a field of study derives from the Western Civilization
More informationGravitational Magnetic Force
Gravitational Magnetic Force The curved space-time around current loops and solenoids carrying arbitrarily large steady electric currents is obtained from the numerical resolution of the coupled Einstein-Maxwell
More informationThe Origin of the Visible Mass in the Universe
The Origin of the Visible Mass in the Universe Or: Why the Vacuum is not Empty Ralf Rapp Cyclotron Institute + Physics Department Texas A&M University College Station, USA Cyclotron REU Program 2007 Texas
More informationChapter 46 Solutions
Chapter 46 Solutions 46.1 Assuming that the proton and antiproton are left nearly at rest after they are produced, the energy of the photon E, must be E = E 0 = (938.3 MeV) = 1876.6 MeV = 3.00 10 10 J
More informationLecture 24: Cosmology: The First Three Minutes. Astronomy 111 Monday November 27, 2017
Lecture 24: Cosmology: The First Three Minutes Astronomy 111 Monday November 27, 2017 Reminders Last star party of the semester tomorrow night! Online homework #11 due Monday at 3pm The first three minutes
More informationCosmic Background Radiation
Cosmic Background Radiation The Big Bang generated photons, which scattered frequently in the very early Universe, which was opaque. Once recombination happened the photons are scattered one final time
More information